太阳光谱望远镜散射光初步测定

报告了云南天文台太阳不谱望远镜散射光的测定,用零级光谱测定仪器轮廓的方法得到白光散射光最大为８％,平均为５％,估计光路系统改进后仪器散射光将减少。     

云南天文台太阳光谱望远镜偏振分析器检验

介绍了利用云南天文台水平式太阳光谱仪对太阳光谱望远镜偏振分析器进行检验的情况。检验得到的太阳黑子Ｉ,Ｑ,Ｕ,Ｖ四个斯托克斯轮廓与理论轮廓的特征相近,表明该偏振分析器达到了设计要求,用它可以获得太阳黑子的所有斯托克斯参量。     

云南天文台太阳光谱望远镜加Stokes光电偏振分析器的考虑

云南天文台太阳光谱望远镜是无偏振对称光路系统,经过重新装调望远镜空间分辨率在１”以内,光谱上的空间分辨率在１”～２”,跟踪精度在５ 分钟内１”,以上光学参数达到可以加装Ｓｔｏｋｅｓ 偏振分析器,用于参加２３ 周太阳峰年矢量磁场的光谱轮廓研究     

太阳光谱望远镜鬼线强度测量方法及初步结果

介绍了云台太阳光谱望远镜光栅鬼线强度测量方法。给出了２级光谱罗兰鬼线强度的初步测量结果,为母线强度的０．０４９％,结果表明光栅的质量优良,鬼线对光谱测量的影响非常小,一般情况下在光谱资料处理中可以不必考虑鬼线强度的改正。     

光谱望远镜分辨本领测量方法及初步结果

介绍了云南天文台太阳光谱望远镜分辨本领的照相测量方法,给出了初步测量结果为１００５００,这一结果与它的可达到值３０００００相差较大,对产生的原因进行了分析讨论,认为主要是目前光谱望远镜的光学系统尚未处在正常工作状态。     

太阳光谱望远镜仪器轮廓的测定

报告了太阳光谱望远镜的仪器轮廓的测定方法,用He-Ne单膜激光器测定仪器轮廓,得到半宽为0.049,轮廓对称,理论计算仪器轮廓半宽为0.043,说明仪器设计制造和光学调整是成功的。     

光纤阵列太阳光学望远镜偏振分析器设计

给出了满足光纤阵列太阳光学望远镜(FASOT,Fibre Arrayed Solar Optical Telescope)观测目标的偏振分析器的理论设计.它具有以下特点:(1)具备偏振光学开关功能,使得高偏振测量成为可能;(2)在750nm宽度范围内,对各Stokes偏振参量都具有50%以上的理论偏振测量效率,且总的偏振测量效率高于86.6%.使得观测者在如此宽波长范围内可对多条磁敏谱线同时进行偏振测量;(3)根据所选光球和色球线侧重于对线偏振或圆偏振的测量;(4)对偏振元件的制作工艺以及安装误差等具有相当好的容忍度.以上特性使该偏振分析器成为高性能的偏振测量设备.     

一米新真空红外太阳望远镜多波段光谱仪光谱弯曲分析

在太阳长狭缝光谱观测中,光谱的狭缝方向和色散方向应该分别与CCD探测器的两个边缘平行。但实际上,由于狭缝、光栅、CCD探测器的机械安装精度等原因,会造成他们之间的位置关系不匹配,导致得到的太阳光谱总是存在一定的倾斜和变形。即使有时这些倾斜很微小,也会对太阳光谱的平场计算造成严重影响,从而影响整个光谱数据的处理过程。对抚仙湖1 m新真空红外太阳望远镜多波段光谱仪得到的一组Hα光谱数据的倾斜量做了测量和分析,并讨论了其对太阳光谱平场计算的影响。     

太阳Stokes光谱望远镜的结构及其数据处理方法

云南天文台的太阳Stokes光谱望远镜是一台通过测量磁敏谱线的Stokes参数I,Q,U和V的轮廓来研究太阳磁场精细结构的光谱型矢量磁场测量仪。它利用4个完整的Stokes轮廓所蕴含的丰富信息,完全确定辐射的偏振状态,从而精确地测定太阳黑子区的矢量磁场。文章首先介绍了该望远镜的结构,进而详细地介绍了该望远镜所测量的偏振光谱资料的处理方法。     

Ethane ices in the outer Solar System: Spectroscopy and chemistry

We report recent experiments on ethane ices made at temperatures applicable to the outer Solar System. New near- and mid-infrared data for crystalline and amorphous ethane, including new spectra for a seldom-studied solid phase that exists at 35-55 K, are presented along with radiation-chemical experiments showing the formation of more-complex hydrocarbons.     

Solar Magnetism and the Activity Telescope at HSOS

A new solar telescope system is described, which has been operating at Huairou Solar Observing Station (HSOS), National Astronomical Observatories, Chinese Academy of Sciences (CAS), since the end of 2005. This instrument, the Solar Magnetism and Activity Telescope (SMAT), comprises two telescopes which respectively make measurements of full solar disk vector magnetic field and Hα observation. The core of the full solar disk video vector magnetograph is a birefringent filter with 0.1  bandpass, installed in the tele-centric optical system of the telescope. We present some preliminary observational results of the full solar disk vector magnetograms and Hα filtergrams obtained with this telescope system.     

Design and development of the Advanced Technology Solar Telescope

Led by the National Solar Observatory, plans have been made to design and to develop the Advanced Technology Solar Telescope (ATST). The ATST will be a 4‐m general‐purpose solar telescope equipped with adaptive optics and versatile post‐focus instrumentation. Its main aim will be to achieve an angular resolution of 0.03 arcsec (20 km on the solar surface). The project and the telescope design are briefly described.     

Algorithm Design and Test of the Solar Guide Telescope

The Solar Guide Telescope (SGT), an important solar attitude sensor of the SST (Space Solar Telescope, a space solar observing instrument being developed in China), can accurately produce pointing error signals of the SST for attitude control at high speed. We analyze in detail the error algorithm of the heliocentric coordinates and the edge judging of solar images. The measuring accuracy of ±0.5 arcsec of the SGT is verified by experiments on the tracking of the Sun and by testing a sun simulator. Some factors causing the pointing errors are examined.     

European Solar Telescope: Progress status

In this paper, the present status of the development of the design of the European Solar Telescope is described. The telescope is devised to have the best possible angular resolution and polarimetric performance, maximizing the throughput of the whole system. To that aim, adaptive optics and multi‐conjugate adaptive optics are integrated in the optical path. The system will have the possibility to correct for the diurnal variation of the distance to the turbulence layers, by using several deformable mirrors, conjugated at different heights. The present optical design of the telescope distributes the optical elements along the optical path in such a way that the instrumental polarization induced by the telescope is minimized and independent of the solar elevation and azimuth. This property represents a large advantage for polarimetric measurements. The ensemble of instruments that are planned is also presented (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Solar System Capabilities of the Thirty Meter Telescope

The TMT Project is completing the design of a telescope with a primary mirror diameter of 30 m, yielding ten times more light gathering power than the largest current telescopes. It is being designed from the outset as a system that will deliver diffraction-limited resolution (8, 15 and 70 milliarcsec at 1.2, 2.2 and 10 microns, respectively) and high Strehl ratios over a 30 arcsecond science field with good performance over a 2 arcmin field. Studies of a representative suite of instruments that span a very large discovery space in wavelength (0.3–30 microns), spatial resolution, spectral resolution and field-of-view demonstrate their feasibility and their tremendous scientific potential. Of particular interest for solar system research, one of these will be IRIS (Infrared Imaging Spectrometer), a NIR instrument consisting of a diffraction-limited imager and an integral-field spectrometer. IRIS will be able to investigate structures with dimensions of only a few tens of kilometers at the distance of Jupiter. Two other instruments, NIRES and MIRES (Near- and Mid IR Echelle Spectrographs) will enable high angular, high spectral resolution observations of solar system objects from the ground with sensitivities comparable to space-based missions. The TMT system is being designed for extremely efficient operation including the ability to rapidly switch to observations with different instruments to take advantage of “targets-of-opportunity” or changing conditions. Thus TMT will provide capabilities that will enable very significant solar system science and be highly synergistic with JWST, ALMA and other planned astronomy missions.     

NLST: India's National Large Solar Telescope

This article introduces the new Indian 2 m telescope which has been designed by MT Mechatronics in a detailed conceptual design study for the Indian Institute of Astrophysics, Bangalore. We describe the background of the project and the science goals which shall be addressed with this telescope. NLST is a solar telescope with high optical throughput and will be equipped with an integrated Adaptive Optics system. It is optimized for a site with the kind of seeing and wind conditions as they are expected at a lake site in the Himalayan mountains. The telescope can also be used for certain night time applications. We also give the scientific rationale for this class of telescope (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

太阳随动圆顶的一种实现

介绍了太阳随动圆顶的基本原理和一套太阳圆顶随动系统的具体实现及其关键技术 ,可资将来国内建造太阳随动圆顶参考。     

Reports on Test Observations with the Multi-Channel Solar Telescope

In this paper, we have made a report on the test observations with a Multi-Channel Solar Telescope (MCST), which consists of 60 cm Nine-Channel Solar Telescope (NCST), 35 cm Solar Magnetic Field Telescope (SMFT), 8 cm Full Disc Telescope (FDT), 10 cm Full Disc Magnetic Field Telescope (FDMFT) and 14 cm H telescope. These observations demonstrate that the MCST has the following advantages: (a) It can work at more than nine visible spectral lines simultaneously. In this way, different solar layers of the photosphere and chromosphere can be observed at the same time; (b) every channel of the NCST is entirely equivalent to a videomagnetograph, by means of which the vector magnetic fields and line-of-sight velocity fields can be measured; (c) real-time monochromatic images of the photosphere and chromosphere can be obtained with the FDT, FDMFT, and H Telescope; (d) high-temporal-resolution full-disk magnetic fields can be measured with the FDMFT; (e) spectral profiles over a large field of view can be scanned with the NCST.